Understanding Our Universe
3rd Edition
ISBN: 9780393614428
Author: PALEN, Stacy, Kay, Laura, Blumenthal, George (george Ray)
Publisher: W.w. Norton & Company,
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Chapter 5, Problem 42QAP
To determine
The drop in the sun’s brightness if the Jupiter passes in front of the sun as observed by the alien astronomer.
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The angular separation in degrees of two objects is (physical separation × 360°) / (2 π × distance). If an individual was observing our solar system from Castor at a distance of 10.2 light years. What angular resolution, in arcsecond, is needed to resolve the Sun-Jupiter system (5.46 AU) as distinct points of light?
Light from the sun takes 8 minutes to reach earth. How long does it take to reach Neptune?
If a transit depth of 0.001 (or 0.1% decrease in brightness) is detected for a star with a radius of 0.3 RSun, what would the radius of the exoplanet be in units of RSun?
Chapter 5 Solutions
Understanding Our Universe
Ch. 5.1 - Prob. 5.1CYUCh. 5.2 - Prob. 5.2CYUCh. 5.3 - Prob. 5.3CYUCh. 5.4 - Prob. 5.4CYUCh. 5.5 - Prob. 5.5CYUCh. 5.6 - Prob. 5.6CYUCh. 5 - Prob. 1QAPCh. 5 - Prob. 2QAPCh. 5 - Prob. 3QAPCh. 5 - Prob. 4QAP
Ch. 5 - Prob. 5QAPCh. 5 - Prob. 6QAPCh. 5 - Prob. 7QAPCh. 5 - Prob. 8QAPCh. 5 - Prob. 9QAPCh. 5 - Prob. 10QAPCh. 5 - Prob. 11QAPCh. 5 - Prob. 12QAPCh. 5 - Prob. 13QAPCh. 5 - Prob. 14QAPCh. 5 - Prob. 15QAPCh. 5 - Prob. 16QAPCh. 5 - Prob. 17QAPCh. 5 - Prob. 18QAPCh. 5 - Prob. 19QAPCh. 5 - Prob. 20QAPCh. 5 - Prob. 21QAPCh. 5 - Prob. 22QAPCh. 5 - Prob. 23QAPCh. 5 - Prob. 24QAPCh. 5 - Prob. 25QAPCh. 5 - Prob. 27QAPCh. 5 - Prob. 28QAPCh. 5 - Prob. 29QAPCh. 5 - Prob. 30QAPCh. 5 - Prob. 31QAPCh. 5 - Prob. 32QAPCh. 5 - Prob. 34QAPCh. 5 - Prob. 35QAPCh. 5 - Prob. 36QAPCh. 5 - Prob. 37QAPCh. 5 - Prob. 38QAPCh. 5 - Prob. 39QAPCh. 5 - Prob. 40QAPCh. 5 - Prob. 41QAPCh. 5 - Prob. 42QAPCh. 5 - Prob. 43QAPCh. 5 - Prob. 44QAPCh. 5 - Prob. 45QAP
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- Why were giant planets close to their stars the first ones to be discovered? Why has the same technique not been used yet to discover giant planets at the distance of Saturn?arrow_forwardWhy is it hard to give exact diameters for even the larger objects in the Kuiper belt?arrow_forwardUsing a 8-m reflector telescope on Mars, what is the maximum distance we could measure using stellar parallax?arrow_forward
- Why is Neptune a deep blue color?arrow_forwardIf a transit depth of 0.00001 can be detected with the Kepler spacecraft, what is the smallest planet that could be detected around a 0.3 RsunM dwarf star?arrow_forwardWhy are young Jupiters easier to see with direct imaging than old Jupiters?arrow_forward
- If an individual was observing our solar system from Castor at a distance of 6.0 light years. What angular resolution in arcsecond is needed to resolve the Sun- earth system as distinct points of lightarrow_forwardMercury is approximately 0.4 AU away from the Sun, whereas Neptune is approximately 30 AU away from the Sun. How long does it take light to reach Mercury and Neptune from the Sun?arrow_forwardIf asteroid Toutatis were to pass somewhere within 24 x105 km of planet Syrene, what is the probability that it would strike the Syrene? Calculate the probability by considering an imanginary dartboard of radius 24 x105 km in which the bulls-eye has Syrene's radius, 6500.0 km. Assume the radius of Toutatis is much smaller than the radius of Syrene.arrow_forward
- In Saturns rings, each ring particle collides with another particle on average around 4.6 hours. If a ring particle was to survive for that age of the solar system, which 4.6 x109 years, how many collisions would it undergo? Assume there are 365.25 days in a year.arrow_forwardNeed asap.. If you increase the semi-major axis of an exoplanet's orbit, how does this affect the radial velocity signal of the host star? (A).The amplitude of the radial velocity curve increases. or (B). The amplitude of the radial velocity curve decreases.arrow_forwardAnalysis of the spectrum of a solar–mass star shows a periodic back-and-forth shift of its spectral lines with a period of 3 days. A spectral line centred at wavelength λ0 = 500 nm shows a shift ∆λ = ±2.5 × 10−4 nm. Estimate the mass of the unseen orbiting companion by assuming the angle of inclination i = 90◦, and express your answer in Jupiter masses.arrow_forward
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